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Extragalactic Background Fluctuation from the Numerical Galaxies

Extragalactic Background Fluctuation from the Numerical Galaxies. Hideki Yahagi DTAP, NAOJ Masahiro Nagashima Univ. of Durham Yuzuru Yoshii IoA, Univ. of Tokyo. Cosmic Background Radiation. Hauser & Dwek (2002). WMAP. Cosmic Microwave Background. Benett et al. (2003). ISO.

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Extragalactic Background Fluctuation from the Numerical Galaxies

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  1. Extragalactic Background Fluctuationfromthe Numerical Galaxies Hideki Yahagi DTAP, NAOJ Masahiro Nagashima Univ. of Durham Yuzuru Yoshii IoA, Univ. of Tokyo

  2. Cosmic Background Radiation Hauser & Dwek (2002)

  3. WMAP Cosmic Microwave Background Benett et al. (2003)

  4. ISO Cosmic far-IR Background Matsuhara et al. (2000)

  5. ISO Cosmic near-IR Background

  6. νGC = N-body + SAM • Dark matter carries most of mass in the Universe • Galaxies are baryonic components accumulated at the bottom of the potential well generated by dark matter • We can treat the evolution of dark matter distribution (by N-body method) and evolution of galaxies (by Semi-analytic model; SAM) separately • Spatial distribution →N-body • Other observable quantities →SAM • Kauffmann et al. (1999)

  7. Parameters of N-body simulation • Computer:VPP-5000 (@ ADAC/NAOJ) • Number of particles:5123 • Cosmological parameters: W=0.3, l=0.7, s8=1.0 • Box size:70h-1 Mpc • Movie

  8. Effective mass resolution is several 1010M8 (L = 70h-1Mpc) Well-fitted by Sheth-Tormen type mass function Mass Function of Dark Halos Yahagi, Nagashima, and Yoshii (2003)

  9. Nagashima et al. (2001) Semi-Analytic Model

  10. Semi-Analytic Model

  11. Semi-Analytic Model

  12. Semi-Analytic Model

  13. Semi-Analytic Model

  14. z=0 Distribution of Dark Matter and Galaxies

  15. Cluster at z=0 Distribution and Colors ofGalaxies in the Cluster

  16. Cluster @z=0.5 Distribution and Colors ofGalaxies in the Cluster

  17. Cluster at z=1 Distribution and Colors ofGalaxies in the Cluster

  18. Angular correlation function of galaxies Yahagi, Nagashima, Miyazaki, Gouda, & Yoshii Extragalactic background fluctuation Nagashima, Yahagi, & Yoshii Cosmic string search Japanese Virtual Observatory groups Applications of νGC

  19. Wedge diagram Angular Correlation Function 40x40 arcmin2 RC<22 22<RC<24 24<RC<26 26<RC

  20. Field-to-field variation Angular Correlation Function （DD-2DR+RR)/RR(Landy & Szalay 1993)

  21. Integral Constraints Angular Correlation Function 1+wtrue=<1+wtrue> =<1+wobs><(n/<n>)2 > ~1+<wobs>+σ2

  22. Limiting magnitude Angular Correlation Function

  23. Angular Correlation Function • Subaru Suprime-Cam • GTO 2.2 deg2 field • S. Miyazaki (Subaru telescope, NAOJ)et al. Subaru Telescope (National Astronomical Observatory of Japan) Suprime-Cam (National Astronomical Observatory)

  24. Comparison with observational data Angular Correlation Function

  25. Two-body correlation function of galaxies Correlation function of galaxies brighter than the limiting magnitude Edxtra-galactic background fluctuation Correlation function of galaxies dimmer than the limiting magnitude Extragalactic Background Fluctuation

  26. Diffuse extra-galactic background light (EBL) Superposition of unresolved galaxies ?(NIR) Expected outcome from EBL anisotropy Source of EBL Number of unresolved galaxies IR Satellite projects SIRTF Astro-F, SPICA Extragalactic Background Fluctuation

  27. Extragalactic Background Fluctuation

  28. Extragalactic Background Fluctuation

  29. Kashlinsky et al. (2002) Extragalactic Background Fluctuation

  30. Summary • N-body + SAM = νGC • High mass resolution • Parallelized AMR N-body simulation code • Comparison with observation • Angular correlation function • Our catalog realizes the observational data • Extragalactic background light • Our catalog fits the 2MASS results quite well • What is the origin of the excess at 10mins<?

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